For a detailed description of spectral scans and line identification, data processing and calibration, the reader is referred to the Supplementary Material accompanying a paper submitted to Science in March 2013 entitled: "Isotope Ratios of H, C and O in Martian Atmospheric Water and Carbon Dioxide Measured by the Curiosity Rover", by Chris R. Webster, Paul R. Mahaffy, Gregory J. Flesch, Paul B. Niles, John H. Jones, Laurie A. Leshin, Sushil K. Atreya, Jennifer C. Stern, Lance E. Christensen, Toby Owen, Heather Franz, and the MSL Science Team.  This document is also available on request. 
For Evolved Gas Analysis (EGA) runs, further details are given in a companion Science paper authored by Laurie Leshin et al. in the same volume.  Briefly, ingested solid sample is heated in a pyrolysis oven whose gaseous products are routed to either QMS, TLS or GC in a helium gas flow.  For any EGA run, TLS is given a "temperature cut" where the effluent is delivered to the TLS Herriott cell during a certain oven temperature portion of its heating ramp, typically a 50-100 deg C cut that may be at lower or higher temperature, and identified in our level 2 data set.  Isotopic ratios for d17O and d13C18O, while provided for standard "atmospheric" runs, cannot be retrieved meaningful values for EGA runs where spectral signals (line depths) are much weaker.
Rocknest EGA effluent gases were observed by the QMS to contain contamination from a derivatization agent MTBSTFA that was taken along with the SAM experiment.  For TLS, numerous underlying spectral lines were observed in our spectral scans whose contribution to the CO2 and H2O isotopic lines could not be unambiguously identified.  However, these interferences were generally small, and diminished throughout the Rocknest run series.
For EGA analysis, it is important to take into account what gases and isotope ratios would result with NO sample in the pyrolysis oven.  To that end, the EGA run is duplicated in this condition (no sample) and minor amounts of both CO2 and H2O are produced and detected in TLS.  Because these "blank cup" gases are measured by TLS to have isotopic ratios different from the Mars solid samples, we have made corrections to the level 2 data based on a blank cup analysis. These corrections are described in Leshin et al. Science, submitted 2013.
Isotope ratios given refer to SMOW for oxygen isotopes and VPDB for 13C ratios. These ratios were determined using identical data processing software in comparison to certified calibration gas or liquid standards determined by IRMS.  
In some cases (entries marked with "x") scientifically useful data was not retrieved due to instrumentation issues such as fast moving spectral scans or poor signal-to-noise ratios. 
All isotope delta values and their standard errors (one-sigma, SE) are given in "per mil" according to standard convention. 
In most cases, values for d13C, d18O and d17O values result from the mean value from the two spectral regions 1 and 2 accessed by a single laser by changing the laser temperature. Values for d13C18O multiple isotope come only from Region 2.
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This dataset is from a third evolved gas sample from the Rocknest site.
The temperature cut for this run was 234-425.
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